Psi5 Aurigae

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For other star systems with this Bayer designation, see Psi Aurigae.
Psi5 Aurigae
Diagram showing star positions and boundaries of the Auriga constellation and its surroundings
Cercle rouge 100%.svg

The location of ψ5 Aurigae (circled)
Observation data
Epoch J2000      Equinox J2000
Constellation Auriga
Right ascension 06h 46m 44.3388s[1]
Declination +43° 34′ 38.737″[1]
Apparent magnitude (V) 5.25[2]
Spectral type G0 V[3]
U−B color index +0.06[2]
B−V color index +0.570[4]
Radial velocity (Rv) –24[5] km/s
Proper motion (μ) RA: –1.07[1] mas/yr
Dec.: +164.25[1] mas/yr
Parallax (π) 60.56 ± 0.73[1] mas
Distance 53.9 ± 0.6 ly
(16.5 ± 0.2 pc)
Absolute magnitude (MV) 4.13[5]
Mass 1.079[6] M
Radius 1.18[6] R
Surface gravity (log g) 4.06[3] cgs
Temperature 5,989[3] K
Metallicity [Fe/H] +0.05[3] dex
Rotational velocity (v sin i) 5.03[4] km/s
Age 3.2[5] Gyr
Other designations
56 Aurigae, ADS 5425, BD+43°1595, FK5 255, HD 48682, HIP 32480, HR 2483, SAO 41330.[7]

Psi5 Aurigae5 Aur, ψ5 Aurigae) is the Bayer designation for a star[8] in the northern constellation of Auriga. It is faintly visible to the naked eye with an apparent visual magnitude of 5.25.[2] Based upon parallax measurements made during the Hipparcos mission, this star is approximately 53.9 light-years (16.5 parsecs) distant from Earth.[1] There is an optical companion[8] which is 36 arcseconds away and has an apparent magnitude of +8.4.

The spectrum of this star shows it to be a G-type main sequence star with a stellar classification of G0 V.[3] Thought to be around 4 billion years old, it is similar in size, mass,[6] and composition to the Sun,[3] making this a solar analog. It is radiating energy into space at an effective temperature of 5,989 K,[3] giving it the golden-hued glow of a G-type star.[9]

Observation in the infrared shows an excess emission that suggests the presence of a circumstellar disk of dust, known as a debris disk. This material has a mean temperature of 60 K, indicating that it is orbiting at a distance of about 29 astronomical units from the host star. The dust has about half the mass of the Moon and is around 600 million years old.[10] The star is being examined for evidence of extrasolar planets,[11] but none have been found so far.


  1. ^ a b c d e f van Leeuwen, Floor (November 2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv:0708.1752v1free to read, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357.  Note: see VizieR catalogue I/311.
  2. ^ a b c Argue, A. N. (1966), "UBV photometry of 550 F, G and K type stars", Monthly Notices of the Royal Astronomical Society, 133: 475, Bibcode:1966MNRAS.133..475A, doi:10.1093/mnras/133.4.475. 
  3. ^ a b c d e f g Cenarro, A. J.; et al. (January 2007), "Medium-resolution Isaac Newton Telescope library of empirical spectra - II. The stellar atmospheric parameters", Monthly Notices of the Royal Astronomical Society, 374 (2): 664–690, arXiv:astro-ph/0611618free to read, Bibcode:2007MNRAS.374..664C, doi:10.1111/j.1365-2966.2006.11196.x. 
  4. ^ a b Martínez–Arnáiz, R.; et al. (September 2010), "Chromospheric activity and rotation of FGK stars in the solar vicinity. An estimation of the radial velocity jitter", Astronomy and Astrophysics, 520: A79, arXiv:1002.4391free to read, Bibcode:2010A&A...520A..79M, doi:10.1051/0004-6361/200913725. 
  5. ^ a b c Holmberg, J.; Nordström, B.; Andersen, J. (July 2009), "The Geneva-Copenhagen survey of the solar neighbourhood. III. Improved distances, ages, and kinematics", Astronomy and Astrophysics, 501 (3): 941–947, arXiv:0811.3982free to read, Bibcode:2009A&A...501..941H, doi:10.1051/0004-6361/200811191. 
  6. ^ a b c Takeda, Genya; et al. (February 2007), "Structure and Evolution of Nearby Stars with Planets. II. Physical Properties of ~1000 Cool Stars from the SPOCS Catalog", The Astrophysical Journal Supplement Series, 168 (2): 297–318, arXiv:astro-ph/0607235free to read, Bibcode:2007ApJS..168..297T, doi:10.1086/509763. 
  7. ^ "56 Aur -- Star in double system", SIMBAD Astronomical Database, Centre de Données astronomiques de Strasbourg, retrieved 2012-08-24. 
  8. ^ a b Eggleton, P. P.; Tokovinin, A. A. (September 2008), "A catalogue of multiplicity among bright stellar systems", Monthly Notices of the Royal Astronomical Society, 389 (2): 869–879, arXiv:0806.2878free to read, Bibcode:2008MNRAS.389..869E, doi:10.1111/j.1365-2966.2008.13596.x. 
  9. ^ "The Colour of Stars", Australia Telescope, Outreach and Education, Commonwealth Scientific and Industrial Research Organisation, December 21, 2004, retrieved 2012-01-16. 
  10. ^ Rodriguez, David R.; Zuckerman, B. (February 2012), "Binaries among Debris Disk Stars", The Astrophysical Journal, 745 (2): 147, arXiv:1111.5618free to read, Bibcode:2012ApJ...745..147R, doi:10.1088/0004-637X/745/2/147. 
  11. ^ Grether, Daniel; Lineweaver, Charles H. (April 2006), "How Dry is the Brown Dwarf Desert? Quantifying the Relative Number of Planets, Brown Dwarfs, and Stellar Companions around Nearby Sun-like Stars", The Astrophysical Journal, 640 (2): 1051–1062, arXiv:astro-ph/0412356free to read, Bibcode:2006ApJ...640.1051G, doi:10.1086/500161. 

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